1. INTRODUCTION

The determination of redshifts of galaxies in distant clusters has been
at a standstill since the summary paper of
Humason, Mayall, and
Sandage (1956)
was published. In
that paper redshifts up to 61,000 km s-1 or z = 0.2025
were reported. Since that time
larger redshifts have been determined only for galaxies with strong
emission lines and
which, therefore, may not be normal. One of the most difficult
accomplishments in the
last 10 years was the determination of the redshift of
3C 295 by
Minkowski (1960) by
identifying the most obvious feature of the spectrum with the emission
line 3727 of [O II].
Schmidt (1965)
has determined redshifts greater than 0.2 for
several radio galaxies with strong emission lines.

As far as normal galaxies are concerned, the limiting magnitude reached
of V 17.4
is presumably due to the fact that such galaxies are extended objects
and the sky brightness
is so great that photographic spectra are completely dominated by the
sky spectrum.
Image-tube spectrographs decrease the time it takes to obtain a
spectrum, but do not
improve the contrast of the galaxy spectrum against that of the sky.

Several attempts to determine redshifts greater than 0.2 have been
made. A number of these are discussed by
Zwicky (1959).
Of particular interest was the work of
Baum (1962),
who measured broad-band colors from 3730 to 9875 Å, calibrated them
absolutely in terms of flux, and then determined the redshift by fitting
the derived fluxes to
the corresponding broad-band fluxes for nearby galaxies. He was
successful in this and has published several redshifts
(Baum 1962).
Because the bandpasses were large, the
inherent accuracy was not high. Also, the data were not sufficient to
determine whether the galaxy energy distribution was normal.

Several years ago it was realized that the only practical way to
determine large
redshifts was to use a technique in which the sky background was
subtracted accurately.
A star-sky chopping system coupled with pulse-counting electronics had
been used
successfully in the prime-focus spectrum scanner for many years and was
an obvious
technique to use. With the determination of large redshifts of distant
galaxies as the
prime motive, the 32-channel photoelectric spectrometer was designed and
built
(Oke 1969).
This instrument is now being used regularly for work on very
faint objects; some early results are reported below.
Gunn (1971)
has also reported on similar work of this kind.